Stellar Evolution with Rotation V: Changes in all the Outputs of Massive Star Models

TL;DR

This paper presents comprehensive models of rotating massive stars, incorporating detailed physics to analyze how rotation affects their evolution, surface composition, and lifetimes, providing insights into stellar behavior at different masses.

Contribution

It introduces advanced rotating star models with detailed physics, showing rotation's effects are comparable to mass loss and significantly alter stellar evolution and surface composition.

Findings

Rotation extends main sequence lifetime by up to 30%

Rotation causes surface He and N enhancements, especially in higher mass stars

Effects of rotation are comparable to mass loss in massive stars

Abstract

Grids of models for rotating stars are constructed in the range of 9 to 120 M$_{\odot}$ at solar metallicity. The following effects of rotation are included: shellular rotation, new structure equations for non-conservative case, surface distorsions, increase of mass loss with rotation, meridional circulation and interaction with horizontal turbulence, shear instability and coupling with thermal effects, advection and diffusion of angular momentum treated in the non-stationary regime, transport and diffusion of the chemical elements. Globally we find that for massive stars the effects of rotation have an importance comparable to those of mass loss. For an average rotation, the tracks in the HR diagram are modified like a moderate overshoot would do. In general, an average rotation may increase the MS lifetime up to about 30 %; for the helium-burning phase the effects are smaller and amount to at most 10 %. Rotation also brings significant surface He- and N-enhancements, they are higher for higher masses and rotation.